The physical conditions required for forming the first low mass stars are now understood to be a critical amount of heavy elements and some degree of turbulence to seed fragmentation. However, the transition from Population III to Population II has yet to be characterized in a global context. The process of external enrichment, in which a star-less halo is promptly enriched by the blast-wave...
Metals from Population III (Pop III) supernovae led to the formation of less massive Pop II stars in the early universe, altering the course of evolution of primeval galaxies and cosmological reionization. There are a variety of scenarios in which heavy elements from the first supernovae were taken up into second-generation stars, but cosmological simulations only model them on the largest...
There have been many attempts to investigate the first stars by analysing extremely metal-poor stars. Often, these studies rely on the assumption that the abundances observed in old, extremely metal-poor stars directly correspond to the yields of a single Pop III supernova (SN). We run high-redshift cosmological simulations to test this assumption. In these simulations we model the formation...
